scholarly journals Nonlocal Black Hole Evaporation and Quantum Metric Fluctuations via Inhomogeneous Vacuum Density

2018 ◽  
Vol 2018 ◽  
pp. 1-9 ◽  
Author(s):  
Alexander Y. Yosifov ◽  
Lachezar G. Filipov
Keyword(s):  
Black Hole ◽  
Quantum Information ◽  
Vacuum Energy ◽  
Vacuum Energy Density ◽  
Back Reaction ◽  
Vacuum Fluctuations ◽  
Schwarzschild Black Hole ◽  
Black Hole Background ◽  
Schwarzschild Radius ◽  
Metric Fluctuations

Inhomogeneity of the actual value of the vacuum energy density is considered in a black hole background. We examine the back-reaction of a Schwarzschild black hole to the highly inhomogeneous vacuum density and argue the fluctuations lead to deviations from general relativity in the near-horizon region. In particular, we found that vacuum fluctuations onto the horizon trigger adiabatic release of quantum information, while vacuum fluctuations in the vicinity of the horizon produce potentially observable metric fluctuations of order of the Schwarzschild radius. Consequently, we propose a form of strong nonviolent nonlocality in which we simultaneously get nonlocal release of quantum information and observable metric fluctuations.

scholarly journals ENTANGLEMENT AND THERMODYNAMICS OF BLACK HOLE ENTROPY

2008 ◽  
Vol 17 (13n14) ◽  
pp. 2549-2553 ◽  
Author(s):  
R. BROUT
Keyword(s):  
Black Hole ◽  
Energy Density ◽  
Vacuum Energy ◽  
Entanglement Entropy ◽  
Black Hole Entropy ◽  
Vacuum Energy Density ◽  
Vacuum Fluctuations ◽  
The Stability

Using simple conditions drawn from the stability of the cosmos in terms of vacuum energy density, the cutoff momentum of entanglement is related to the Planckian mass. In so doing the black hole entropy is shown to be independent of the number of field species that contribute to vacuum fluctuations. And this is in spite of the fact that the number of field species is a linear multiplicand of the entanglement entropy when the latter is expressed in terms of the fundamental momentum cutoff of all fields.

scholarly journals Black hole S-matrix for a scalar field

2021 ◽  
Vol 2021 (7) ◽  
Author(s):  
Panos Betzios ◽  
Nava Gaddam ◽  
Olga Papadoulaki
Keyword(s):  
Black Hole ◽  
Normal Modes ◽  
Massless Scalar ◽  
Scattering Process ◽  
Schwarzschild Black Hole ◽  
Asymptotically Flat ◽  
Scalar Particles ◽  
Black Hole Background ◽  
S Matrix ◽  
Do So

Abstract We describe a unitary scattering process, as observed from spatial infinity, of massless scalar particles on an asymptotically flat Schwarzschild black hole background. In order to do so, we split the problem in two different regimes governing the dynamics of the scattering process. The first describes the evolution of the modes in the region away from the horizon and can be analysed in terms of the effective Regge-Wheeler potential. In the near horizon region, where the Regge-Wheeler potential becomes insignificant, the WKB geometric optics approximation of Hawking’s is replaced by the near-horizon gravitational scattering matrix that captures non-perturbative soft graviton exchanges near the horizon. We perform an appropriate matching for the scattering solutions of these two dynamical problems and compute the resulting Bogoliubov relations, that combines both dynamics. This allows us to formulate an S-matrix for the scattering process that is manifestly unitary. We discuss the analogue of the (quasi)-normal modes in this setup and the emergence of gravitational echoes that follow an original burst of radiation as the excited black hole relaxes to equilibrium.

CAN WE DIFFERENTIATE NEUTRINOS FROM ANTI-NEUTRINOS IN EVOLUTION OF MASSLESS DIRAC FIELDS IN SCHWARZSCHILD BLACK-HOLE BACKGROUND?

2006 ◽  
Vol 21 (07) ◽  
pp. 593-601
Author(s):  
JILIANG JING
Keyword(s):  
Black Hole ◽  
Decay Rate ◽  
Power Law ◽  
Quasinormal Modes ◽  
Tail Behavior ◽  
Schwarzschild Black Hole ◽  
Dirac Fields ◽  
Black Hole Background ◽  
Opposite Chirality

We study analytically the evolution of massless Dirac fields in the background of the Schwarzschild black hole. It is shown that although the quasinormal frequencies are the same for opposite chirality with the same |k|, we can differentiate neutrinos from anti-neutrinos in evolution of the massless Dirac fields provided we know both stages for the quasinormal modes and the power-law tail behavior since the decay rate of the neutrinos is described by t-(2|k|+1) while anti-neutrinos is t-(2|k|+3).

scholarly journals NUMERICAL SIMULATION OF QUASI-NORMAL MODES IN TIME-DEPENDENT BACKGROUND

2004 ◽  
Vol 19 (03) ◽  
pp. 239-252 ◽  
Author(s):  
LI-HUI XUE ◽  
ZAI-XIONG SHEN ◽  
BIN WANG ◽  
RU-KENG SU
Keyword(s):  
Numerical Simulation ◽  
Black Hole ◽  
Wave Propagation ◽  
Normal Modes ◽  
Time Dependent ◽  
Massless Scalar ◽  
Scalar Wave ◽  
Schwarzschild Black Hole ◽  
Black Hole Background ◽  
Scattering Potential

We study the massless scalar wave propagation in the time-dependent Schwarzschild black hole background. We find that the Kruskal coordinate is an appropriate framework to investigate the time-dependent spacetime. A time-dependent scattering potential is derived by considering dynamical black hole with parameters changing with time. It is shown that in the quasinormal ringing both the decay time-scale and oscillation are modified in the time-dependent background.

scholarly journals INSTABILITY OF THE BLACK HOLE HORIZON WITH RESPECT TO ELECTROMAGNETIC EXCITATIONS

2009 ◽  
Vol 18 (14) ◽  
pp. 2351-2356 ◽  
Author(s):  
ALEXANDER BURINSKII
Keyword(s):  
Black Hole ◽  
Exact Solutions ◽  
Maxwell Equations ◽  
Information Loss ◽  
Black Hole Horizon ◽  
Back Reaction ◽  
Vacuum Fluctuations

Analyzing exact solutions to the Einstein–Maxwell equations in the Kerr–Schild formalism, we show that the black hole horizon is unstable with respect to electromagnetic excitations. Contrary to perturbative smooth harmonic solutions, the exact solutions for electromagnetic excitations on the Kerr background are accompanied by singular beams which have very strong back-reaction to the metric and break the horizon, forming the holes which allow radiation to escape from the interior of the black hole. As a result, even the weak vacuum fluctuations break the horizon topologically, covering it by a set of fluctuating microholes. We conclude with a series of nontrivial consequences, one of which is that there is no information loss inside of the black hole.

scholarly journals Quantum corrections to the accretion onto a Schwarzschild black hole in the background of quintessence

2020 ◽  
Vol 80 (12) ◽  
Author(s):  
Kourosh Nozari ◽  
Milad Hajebrahimi ◽  
Sara Saghafi
Keyword(s):  
Black Hole ◽  
Quantum Fluctuations ◽  
Radial Component ◽  
Quantum Corrections ◽  
Back Reaction ◽  
Late Time ◽  
Candidate Model ◽  
Schwarzschild Black Hole ◽  
Singularity Point ◽  
Quintessence Field

AbstractIt is well known that quantum effects may lead to removal of the intrinsic singularity point of back holes. Also, the quintessence scalar field is a candidate model for describing late-time acceleration expansion. Accordingly, Kazakov and Solodukhin considered the existence of back-reaction of the spacetime due to the quantum fluctuations of the background metric to deform a Schwarzschild black hole, which led to a change of the intrinsic singularity of the black hole to a 2-sphere with a radius of the order of the Planck length. Also, Kiselev rewrote the Schwarzschild metric by taking into account the quintessence field in the background. In this study, we consider the quantum-corrected Schwarzschild black hole inspired by Kazakov–Solodukhin’s work, and the Schwarzschild black hole surrounded by quintessence deduced by Kiselev to study the mutual effects of quantum fluctuations and quintessence on the accretion onto the black hole. Consequently, the radial component of the 4-velocity and the proper energy density of the accreting fluid have a finite value on the surface of its central 2-sphere due to the presence of quantum corrections. Also, by comparing the accretion parameters in different kinds of black holes, we infer that the presence of a point-like electric charge in the spacetime is somewhat similar to some quantum fluctuations in the background metric.

scholarly journals Bound states and decay times of fermions in a Schwarzschild black hole background

2005 ◽  
Vol 72 (10) ◽  
Author(s):  
Anthony Lasenby ◽  
Chris Doran ◽  
Jonathan Pritchard ◽  
Alejandro Caceres ◽  
Sam Dolan
Keyword(s):  
Black Hole ◽  
Bound States ◽  
Schwarzschild Black Hole ◽  
Black Hole Background ◽  
Decay Times

scholarly journals Quintessence and effective AdS brane geometries

2015 ◽  
Vol 30 (13) ◽  
pp. 1550065 ◽  
Author(s):  
K. Priyabrat Pandey ◽  
Abhishek K. Singh ◽  
Sunita Singh ◽  
Supriya Kar
Keyword(s):  
Black Hole ◽  
Energy Density ◽  
Extra Dimension ◽  
Vacuum Energy ◽  
Bound State ◽  
Second Order ◽  
The Other ◽  
Vacuum Energy Density ◽  
Curvature Scalar

A geometric torsion dynamics leading to an effective curvature in a second-order formalism on a D4-brane is revisited with a renewed interest. We obtain two effective AdS 4 brane geometries on a vacuum created pair of [Formula: see text]-brane. One of them is shown to describe an AdS Schwarzschild spinning black hole and the other is shown to describe a spinning black hole bound state. It is argued that a D-instanton in a vacuum created anti-D3-brane within a pair may describe a quintessence. It may seem to incorporate a varying vacuum energy density in a brane universe. We consider the effective curvature scalar on S1 × S1 to analyze torsionless geometries on a vacuum created pair of [Formula: see text]-brane. The emergent AdS 3 brane is shown to describe a Schwarzschild and a Reissner–Nordstrom (RN) geometries in the presence of extra dimension(s).

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